You can create some (but not all) radioisotopes through “photoproduction,” in which the bombarding particles are photons, or by irradiation with stable particles, such as electrons or ionized nuclei. It is a question of the energies involved.
You used to have, in your home, one or more electron accelerators. They were called “cathode ray tubes” and were most commonly used for televisions and computer monitors, before flat-panel displays were affordable. Those devices contained a large vacuum tube, with a metal filament at the back hot enough that thermal electrons could leak off into the vacuum, where they were accelerated towards the screen with an energy of a few kilo-electron-volts, or keV. The kilovolt electronics were why televisions had lots of “do not disassemble” warnings on them, and the electron steering in the vacuum is why your TV went wonky if you held a magnet nearby.
Kilo-eV electrons make x-rays when they stop, which is why your TV had heavy leaded glass in front of the display phosphor. A very similar electron accelerator with energies above about ten mega-eV has enough energy to knock a proton or a neutron out of its nucleus. The threshold is called the “separation energy” of the proton or neutron, and is tabulated in various references. If you change the number of protons or neutrons in a nucleus, it is now a different isotope or a different element, and the odds are good that it is radioactive.
I would consider “irradiating with an electron beam” to be a special case of “shooting full of electricity.” It’s slightly easier if you stop the electrons and collect the high-energy x-rays, since then you can have your irradiated sample outside of your vacuum chamber.
As another poster writes, you can’t do this transmutation via chemical means because the energies involved are too small. Electron ionization energies (or “electron separation energies,” to emphasize the parallel) are typically a few electron-volts, a tiny fraction of the mega-eV required to separate a nucleon. Thermal energies are milli-eV. Even at the temperatures and pressures in the core of the Sun, most nuclei don’t undergo nucleon-exchange reactions; this is why the hydrogen in the Sun’s core will last for ten billion years.